Spherical tensor approach to the solution of the mantle stress problem     

Ondřej Čadek  Reviewer M. Pick  Reviewer J. Šílený 《Studia Geophysica et Geodaetica》1989,33(2):177-197

Summary The technique of spherical tensors is applied to the problem of stress in the mantle. An efficient method for stress computation is developed for the Newtonian mantle with spherical boundaries assuming that the density and gravitational potential in the form of harmonic expansions are known. The ways of including more complicated rheological models as well as the non-spherical shape of boundaries are outlined.

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¶rt; m¶rt; ama anu amuu, m a a nuuu annaama uuauu m. ¶rt;naam, m au nmmu uaumau nmuaa n uu u um u m amu n¶rt;mam u¶rt;m uuuauau. ¶rt; mu u m¶rt;a a a uu ¶rt; u u au.

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Normal gravity model of phobos     

Milan Burša  Reviewer M. Pick 《Studia Geophysica et Geodaetica》1989,33(2):109-116

Summary The normal gravity field of Phobos defined by the sum a) of the gravitational potential of a homogeneous tri-axial ellipsoid representing the body of Phobos, b) of the potential of its centrifugal forces, c) of the constant part in the tidal-forming potential due to Mars, has been investigated. The radius-vector of the equipotential surface representing the normal model, as well as the gravity on it, have been derived. The long-term variations in the figure parameters and in gravity, due to the tidal evolution of the Mars—Phobos system, have been derived.

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¶rt;m a n u mmu a, ¶rt;a a) nmuaa ¶rt;¶rt; m unu¶rt;a, n¶rt;ma m a, ) nmuaa m u, ) nm amu nuua nmuaa m aa. ¶rt; au a¶rt;ua-ma nmu, n¶rt;ma ¶rt;a a ¶rt;, u u u mmu a n¶rt;. auauu naam u u u u mmu, a nuu u um a—.

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The quasi-isotropic relative structure of a geodetic net and the procedure used to establish it     

Lubomír Kubáček  Ján Pecár  Matej Klobušiak  Peter Barica  Reviewer P. Kratochvíl  Reviewer M. Pick 《Studia Geophysica et Geodaetica》1988,32(2):117-128

Summary The method of computing the quasi-isotropic relative structure (QIRS) of a geodetic net which maximizes the relative accuracy between a priori determined points of the net, the configuration of the net being taken into account, is described. The iteration procedure is used to establish this structure.

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nuam n aamu auumn mum naa uu¶rt;u mu, m nu¶rt;um au mum mmu ¶rt; ¶rt;au naau nm m uauu¶rt;u mu. nm umamu m¶rt; uu.

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Modification of the Runcorn's equations on convection flows     

Miloš Pick  Ivanka Charvátová-Jakubcová  Reviewer O. Novotný 《Studia Geophysica et Geodaetica》1988,32(1):47-53

Summary Runcorn's equations, which can be used to compute the stresses caused by convection flows from the outer gravity field, were transformed so that gravity anomalies or geoid heights can be employed as input data.

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au aa, m n¶rt;m u n u mmu u anu, a uu nmau, u maua ma, m unam u¶rt; ¶rt; ¶rt;a, aauu u mmu uu mu¶rt;a.

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Gravity topographic corrections computed from a square grid of height points     

Miloš Pick  Reviewer Z. Šimon 《Studia Geophysica et Geodaetica》1988,32(3):245-248

Summary Computation of terrain corrections from a map with a square grid of mean height points

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uu mnauu nna n am ¶rt;u m u¶rt; a¶rt;am mu m nm.

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On determination of shape of earth by using analytical continuation of function     

Miloš Pick 《Studia Geophysica et Geodaetica》1965,9(3):219-224

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A note on upper limits for hypothetic variation in the Newtonian constant of gravitation     

Milan Burša  Reviewer M. Pick 《Studia Geophysica et Geodaetica》1984,28(4):360-363

Summary It has been demonstrated on the basis of recent astronomical, satellite and LLR data that the variations in the Newtonian constant of gravitation, if any, do not exceed5××10 ^–15 cy^–1 of its relative value.

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¶rt;a amuu u nmu a¶rt;u u a auu naa, m auauuaumau nm, u u um, n¶rt;m5×10 ^–15 mmu ^–1 mum au.

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The planetary system and solar-terrestrial phenomena     

Ivanka Jakubcová  Miloš Pick  Reviewer J. Vondrák 《Studia Geophysica et Geodaetica》1986,30(3):224-235

Summary The Sun moves at different distances round the barycentre of the Solar System with different velocities depending on the distribution of the planets. The mean period of the Sun's motion round the barycentre of 11.8627 years and its time variability were observed. A relation between the basic period of 178.4 years and other periods p_i in the Sun's motion (p_i=178.4/i; i=1, 2, ...) was found. The consistency of the periods in the Sun's motion round the barycentre with the periods of different solar-terrestrial phenomena was studied. It seems that the planetary system governs these phenomena.

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n¶rt; ¶rt;u nu¶rt; au a ama um (11,8627 m) u auauu. a a¶rt;a nuua ¶rt; m¶rt;u nu¶rt;au ¶rt;uu a (p_i=178,4/i). mu nu¶rt;a u nma nu¶rt; n¶rt; a - u. na¶rt;u nu¶rt; am, m a uma nam mu u.

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On the calculation of the gravity terrain corrections in Czechoslovakia     

Miloš Pick  Reviewer Z. Šimon 《Studia Geophysica et Geodaetica》1987,31(2):131-144

Summary A calculation of the gravity terrain corrections by computer is proposed.

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¶rt;aam m¶rt; uuu mnauu nna unau uuum muu.

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Secular tidal and nontidal variations in the Earth's rotation     

Milan Burša  Reviewer M. Pick 《Studia Geophysica et Geodaetica》1987,31(3):219-224

Summary On the basis of the angular momentum balance in the Earth — Moon — Sun system and with the use of the observed secular variation in the Moon's mean motion and the variation in the second zonal geopotential harmonic, the tidal and nontidal variations in the angular velocity of the Earth's rotation are computed and different values describing the field of tidal forces estimated.

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¶rt; u au m uma ¶rt;uu um —a—, um n a¶rt;u uu ¶rt; ¶rt;uu u m aauunmuaa nuu u nuu auauu mu au u u ¶rt;am ua a ¶rt;a uu, nuau n u nuu mu.

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